Measurements of the Intensity and Polarization of the Anomalous Microwave Emission in the Perseus molecular complex with QUIJOTE
R. Génova-Santos, J. A. Rubiño-Martín, R. Rebolo, A. Peláez-Santos, C. H. López-Caraballo, S. Harper, R. A. Watson, M. Ashdown, R. B. Barreiro, B. Casaponsa, C.… 展开作者
R. Génova-Santos, J. A. Rubiño-Martín, R. Rebolo, A. Peláez-Santos, C. H. López-Caraballo, S. Harper, R. A. Watson, M. Ashdown, R. B. Barreiro, B. Casaponsa, C. Dickinson, J. M. Diego, R. Fernández-Cobos, K. J. B. Grainge, D. Herranz, R. Hoyland, A. Lasenby, M. López-Caniego, E. Martínez-González, M. McCulloch, S. Melhuish, L. Piccirillo, Y. C. Perrott, F. Poidevin, N. Razavi-Ghods, P. F. Scott, D. Titterington, D. Tramonte, P. Vielva, R. Vignaga
Anomalous microwave emission (AME) has been observed in numerous sky regions, in the frequency range ~10-60 GHz. One of the most scrutinized regions is G159.6-18.5, located within the Perseus molecular complex. In this paper we present further observations of this region (194 hours in total over ~250 deg^2), both in intensity and in polarization. They span four frequency channels between 10 and 20 GHz, and were gathered with QUIJOTE, a new CMB experiment with the goal of measuring the polarization of the CMB and Galactic foregrounds. When combined with other publicly-available intensity data, we achieve the most precise spectrum of the AME measured to date, with 13 independent data points being dominated by this emission. The four QUIJOTE data points provide the first independent confirmation of the downturn of the AME spectrum at low frequencies, initially unveiled by the COSMOSOMAS experiment in this region. We accomplish an accurate fit of these data using models based on electric dipole emission from spinning dust grains, and also fit some of the parameters on which these models depend.
We also present polarization maps with an angular resolution of ~1 deg and a sensitivity of ~25 muK/beam. From these maps, which are consistent with zero polarization, we obtain upper limits of Pi<6.3% and <2.8% (95% C.L.) respectively at 12 and 18 GHz, a frequency range where no AME polarization observations have been reported to date. These constraints are compatible with theoretical predictions of the polarization fraction from electric dipole emission originating from spinning dust grains. At the same time, they rule out several models based on magnetic dipole emission from dust grains ordered in a single magnetic domain, which predict higher polarization levels. Future QUIJOTE data in this region may allow more stringent constraints on the polarization level of the AME.
QUIJOTE Scientific Results. II. Polarisation Measurements of the Microwave Emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44
QUIJOTE scientific results XIX. New constraints on the synchrotron spectral index using a semi-blind component separation method
Instituto de Astrofísica de Canarias（加那利天体物理学研究所）；Universidad de La Laguna（拉古纳大学）；Instituto de Física de Cantabria (IFCA), CSIC-Univ. de Cantabria（坎塔布里亚物理研究所 (IFCA)，西班牙国家研究委员会-坎塔布里亚大学）；University of Cambridge（剑桥大学）
QUIJOTE scientific results -- XIII. Intensity and polarization study of supernova remnants in the QUIJOTE-MFI wide survey: CTB 80, Cygnus Loop, HB 21, CTA 1, Tycho and HB 9
All-sky modeling of Galactic emission at radio and microwave frequencies
The University of Manchester（曼彻斯特大学）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉古纳大学）；University of Oslo（奥斯陆大学）；University of Cambridge（剑桥大学）；University of Oxford（牛津大学）
Discovery of a Perseus-like cloud in the early Universe: HI-to-H2 transition, carbon monoxide and small dust grains at zabs=2.53 towards the quasar J0000+0048
